新西兰天文作业代写 火丁质量

2020-04-01 01:15

由于火星的质量和磁场的缺乏，它有一个独特的大气层。大气可分为四个独立的区域，分别称为外大气层、热层、中间层和对流层。外逸层是最外层的区域，从200公里延伸到与空间融合的模糊半径。在外逸层以下是热层或上层大气，在那里太阳用热辐射轰击气体，产生一层层高温气体。接近火星表面时，热层与中间层在火星表面100公里以上的地方合并。中间层距离火星表面60至100公里。在大气的这一地区，温度或多或少是恒定的。由于热波从行星垂直传播，确实存在温度变化。这些波引起绝热加热和冷却，导致全球热潮。涨潮的幅度随着向上传播而增大。这些波获得振幅，直到垂速变得太高，他们“打破”，导致局部混合。在中间层之下存在着最温暖、最稠密的对流层。由于悬浮的尘埃颗粒吸收了来自太阳的辐射，这一地区相对温暖。对流层的平均递减率为2.5 K km-1。这比干燥绝热空气的递减率还小，这是由于悬浮尘埃的热量所致。15公里以下的对流在大气温度中起着很大的作用。在这个高度以上的温度主要是由太阳辐射决定的。火星大气温度与海拔的关系如图1所示。在这颗红色星球的表面，平均温度为210k。
新西兰天文作业代写 火丁质量
Mars has a unique atmosphere due to the planet’s mass and lack of a magnetic field. The atmosphere can be divided into four separate regions named the exosphere, thermosphere, mesosphere, and troposphere. The exosphere is the outer most region extending from two hundred kilometers until the vague radius at which it blends with space. Below the exosphere is the thermosphere or upper atmosphere where the sun bombards the gasses with thermal radiation causing layers of high temperature gas. Approaching the surface, the thermosphere merges with the mesosphere just above one hundred kilometers above the Martian surface. The mesosphere ranges from sixty to one hundred kilometers above the surface of mars. In this region of the atmosphere the temperature is more or less constant. There do exist variation in temperature due to thermal wave propagating vertically away from the planet. These waves cause adiabatic heating and cooling, leading to global thermal tides. The amplitude of the tides increases as the propagate upwards. These waves gain amplitude until the lapse rate becomes too high and they ‘break’ which leads to local mixing. Below the mesosphere exist the warmest and densest region, the troposphere. This region is relatively warm due to suspended dust particles which absorb radiation from the sun. The average lapse rate in the troposphere is 2.5 K km-1. This is less than the lapse rate of dry adiabatic air due to the heat from suspended dust. Below fifteen kilometers convection plays a large role in the temperature of the atmosphere. Above this altitude temperature is mostly dictated by solar radiation. The relationship of the Martian atmosphere’s temperature as a function of altitude can be seen in Figure 1. (Haberle) At the surface of the red planet the average temperature is 210 K.

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